Gravity and limb-darkening coefficients for compact stars: DA, DB, and DBA eclipsing white dwarfs star

Context. The distribution of the specific intensity over the stellar disk is an essential tool for modeling the light curves in eclipsing binaries, planetary transits, and stellar diameters through interferometric techniques, line profiles in rotating stars, gravitational microlensing, etc. However,...

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Autores: Claret dos Santos, Antonio, Cukanovaite, E., Burdge, K., Tremblay, Pier Emmanuel, Parsons, S., Marsh, T. R.
Formato: artículo
Estado:Versión publicada
Fecha de publicación:2020
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/210795
Acesso em linha:http://hdl.handle.net/10261/210795
Access Level:acceso abierto
Palavra-chave:Binaries: eclipsing
White dwarfs
Stars: evolution
Planetary systems
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dc.title.none.fl_str_mv Gravity and limb-darkening coefficients for compact stars: DA, DB, and DBA eclipsing white dwarfs star
title Gravity and limb-darkening coefficients for compact stars: DA, DB, and DBA eclipsing white dwarfs star
spellingShingle Gravity and limb-darkening coefficients for compact stars: DA, DB, and DBA eclipsing white dwarfs star
Claret dos Santos, Antonio
Binaries: eclipsing
White dwarfs
Stars: evolution
Planetary systems
title_short Gravity and limb-darkening coefficients for compact stars: DA, DB, and DBA eclipsing white dwarfs star
title_full Gravity and limb-darkening coefficients for compact stars: DA, DB, and DBA eclipsing white dwarfs star
title_fullStr Gravity and limb-darkening coefficients for compact stars: DA, DB, and DBA eclipsing white dwarfs star
title_full_unstemmed Gravity and limb-darkening coefficients for compact stars: DA, DB, and DBA eclipsing white dwarfs star
title_sort Gravity and limb-darkening coefficients for compact stars: DA, DB, and DBA eclipsing white dwarfs star
dc.creator.none.fl_str_mv Claret dos Santos, Antonio
Cukanovaite, E.
Burdge, K.
Tremblay, Pier Emmanuel
Parsons, S.
Marsh, T. R.
author Claret dos Santos, Antonio
author_facet Claret dos Santos, Antonio
Cukanovaite, E.
Burdge, K.
Tremblay, Pier Emmanuel
Parsons, S.
Marsh, T. R.
author_role author
author2 Cukanovaite, E.
Burdge, K.
Tremblay, Pier Emmanuel
Parsons, S.
Marsh, T. R.
author2_role author
author
author
author
author
dc.contributor.none.fl_str_mv Ministerio de Economía y Competitividad (España)
Ministerio de Ciencia, Innovación y Universidades (España)
European Commission
European Research Council
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Binaries: eclipsing
White dwarfs
Stars: evolution
Planetary systems
topic Binaries: eclipsing
White dwarfs
Stars: evolution
Planetary systems
description Context. The distribution of the specific intensity over the stellar disk is an essential tool for modeling the light curves in eclipsing binaries, planetary transits, and stellar diameters through interferometric techniques, line profiles in rotating stars, gravitational microlensing, etc. However, the available theoretical calculations are mostly restricted to stars on the main sequence or the giant branch, and very few calculations are available for compact stars. Aims. The main objective of the present work is to extend these investigations by computing the gravity and limb-darkening coefficients for white dwarf atmosphere models with hydrogen, helium, or mixed compositions (types DA, DB, and DBA). Methods. We computed gravity and limb-darkening coefficients for DA, DB, and DBA white dwarfs atmosphere models, covering the transmission curves of the Sloan, UBVRI, Kepler, TESS, and Gaia photometric systems. Specific calculations for the HiPERCAM instrument were also carried out. For all calculations of the limb-darkening coefficients we used the least-squares method. Concerning the effects of tidal and rotational distortions, we also computed for the first time the gravity-darkening coefficients y(lambda) for white dwarfs using the same models of stellar atmospheres as in the case of limb-darkening. A more general differential equation was introduced to derive these quantities, including the partial derivative ( partial differential ln I-o(lambda)/ partial differential ln g)(Teff). Results. Six laws were adopted to describe the specific intensity distribution: linear, quadratic, square root, logarithmic, power-2, and a more general one with four coefficients. The computations are presented for the chemical compositions log[H/He] = -10.0 (DB), -2.0 (DBA) and He/H = 0 (DA), with log g varying between 5.0 and 9.5 and effective temperatures between 3750 and 100 000 K. For effective temperatures higher than 40 000 K, the models were also computed adopting nonlocal thermal equilibirum (DA). The adopted mixing-length parameters are ML2/alpha = 0.8 (DA case) and 1.25 (DB and DBA). The results are presented in the form of 112 tables. Additional calculations, such as for other photometric systems and/or different values of log[H/He], log g, and T-eff can be performed upon request.© ESO 2020
publishDate 2020
dc.date.none.fl_str_mv 2020
2020
2020
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dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/210795
url http://hdl.handle.net/10261/210795
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spelling Gravity and limb-darkening coefficients for compact stars: DA, DB, and DBA eclipsing white dwarfs starClaret dos Santos, AntonioCukanovaite, E.Burdge, K.Tremblay, Pier EmmanuelParsons, S.Marsh, T. R.Binaries: eclipsingWhite dwarfsStars: evolutionPlanetary systemsContext. The distribution of the specific intensity over the stellar disk is an essential tool for modeling the light curves in eclipsing binaries, planetary transits, and stellar diameters through interferometric techniques, line profiles in rotating stars, gravitational microlensing, etc. However, the available theoretical calculations are mostly restricted to stars on the main sequence or the giant branch, and very few calculations are available for compact stars. Aims. The main objective of the present work is to extend these investigations by computing the gravity and limb-darkening coefficients for white dwarf atmosphere models with hydrogen, helium, or mixed compositions (types DA, DB, and DBA). Methods. We computed gravity and limb-darkening coefficients for DA, DB, and DBA white dwarfs atmosphere models, covering the transmission curves of the Sloan, UBVRI, Kepler, TESS, and Gaia photometric systems. Specific calculations for the HiPERCAM instrument were also carried out. For all calculations of the limb-darkening coefficients we used the least-squares method. Concerning the effects of tidal and rotational distortions, we also computed for the first time the gravity-darkening coefficients y(lambda) for white dwarfs using the same models of stellar atmospheres as in the case of limb-darkening. A more general differential equation was introduced to derive these quantities, including the partial derivative ( partial differential ln I-o(lambda)/ partial differential ln g)(Teff). Results. Six laws were adopted to describe the specific intensity distribution: linear, quadratic, square root, logarithmic, power-2, and a more general one with four coefficients. The computations are presented for the chemical compositions log[H/He] = -10.0 (DB), -2.0 (DBA) and He/H = 0 (DA), with log g varying between 5.0 and 9.5 and effective temperatures between 3750 and 100 000 K. For effective temperatures higher than 40 000 K, the models were also computed adopting nonlocal thermal equilibirum (DA). The adopted mixing-length parameters are ML2/alpha = 0.8 (DA case) and 1.25 (DB and DBA). The results are presented in the form of 112 tables. Additional calculations, such as for other photometric systems and/or different values of log[H/He], log g, and T-eff can be performed upon request.© ESO 2020We thank the anonymous referee for helpful comments that have improved the manuscript. The Spanish MEC (AYA2015-71718-R and ESP2017-87676-C5-2-R) is gratefully acknowledged for its support during the development of this work. A.C. also acknowledges financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). The research leading to these results has received funding from the European Research Council under the European Union's Horizon 2020 research and innovation programme n. 677706 (WD3D). This research has made use of the SIMBAD database, operated at the CDS, Strasbourg, France, and of NASA's Astrophysics Data System Abstract Service.Peer reviewedEDP SciencesMinisterio de Economía y Competitividad (España)Ministerio de Ciencia, Innovación y Universidades (España)European CommissionEuropean Research CouncilConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202020202020info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/210795reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2015-71718-Rinfo:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/ESP2017-87676-C5-2-Rinfo:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/SEV-2017-0709info:eu-repo/grantAgreement/EC/H2020/677706http://dx.doi.org/10.1051/0004-6361/201937326Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2107952026-05-22T06:33:51Z
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